| Summary: | 碩士 === 國立臺灣大學 === 天文物理研究所 === 99 === The large photometric surveys, like Pan-STARRS, will provide vast data sets of galaxies and groups to investigate the large-scale structure. While using these data sets, one needs to deal with the large redshift uncertainties. In this thesis, we study the impact of redshift uncertainties to the clustering of galaxies. Using Pan-STARRS light-cone simulation with different redshift errors and sample sizes, we test the performance of a ‘deprojection method’ used to eliminate the redshift distortion from galaxy and group clustering. We find that the deprojection method can recover the real-space correlation function well from photometric samples with area ≥ 4.5 deg2 and redshift error Δz≤ 0.07. For sample covering 2.7 deg2 and 0.9 deg2, this method is valid for Δz≤ 0.03 and Δz≤ 0.01, respectively. We also investigate the mass and color dependence of group clustering for SDSS DR4 group catalogue. Our results show that (1) more massive groups show stronger clustering amplitude, in agreement with previous studies, (2) low-mass groups with blue central galaxies are more strongly clustered than groups with red central galaxies, and (3) for massive groups, groups with red central galaxies are more strongly clustered. We compare our results of color dependence to that obtained by Wang et al. and Berlind et al, and discuss the discrepancy.
|
|---|
